The transient nature of extragalactic type Ia supernovae (SN Ia) prevent studies from conclusively singling out unobserved progenitor configurations [1]}, [2]}, [3]}. It remains fairly certain that the progenitor system of SN Ia comprises at least one compact C\(+\) O white dwarf [4]}, [5]}, [6]}. However, how the state of this primary star reaches a critical point of disruption continues to elude astronomers. This is particularly so given that less than \(\sim \)  15% of locally observed white dwarfs have a mass a few 0.1M\(_{\odot }\)  greater than a solar mass; very few systems near the formal Chandrasekhar-mass limitBy “formal” we are referring to the mass limit that omits stellar rotation (see Appendix of [7]})., M\(_{Ch}\)  \(\approx \)  1.38 M\(_{\odot }\)  [8]}, [9]}, [10]}, [11]}, [12]}.
